2016A&A...586A.138P

Query : 2016A&A...586A.138P

2016A&A...586A.138P - Astronomy and Astrophysics, volume 586A, 138-138 (2016/2-1)

Planck intermediate results. XXXV. Probing the role of the magnetic field in the formation of structure in molecular clouds.

PLANCK COLLABORATION, ADE P.A.R., AGHANIM N., ALVES M.I.R., ARNAUD M., ARZOUMANIAN D., ASHDOWN M., AUMONT J., BACCIGALUPI C., BANDAY A.J., BARREIRO R.B., BARTOLO N., BATTANER E., BENABED K., BENOIT A., BENOIT-LEVY A., BERNARD J.-P., BERSANELLI M., BIELEWICZ P., BOCK J.J., BONAVERA L., BOND J.R., BORRILL J., BOUCHET F.R., BOULANGER F., BRACCO A., BURIGANA C., CALABRESE E., CARDOSO J.-F., CATALANO A., CHIANG H.C., CHRISTENSEN P.R., COLOMBO L.P.L., COMBET C., COUCHOT F., CRILL B.P., CURTO A., CUTTAIA F., DANESE L., DAVIES R.D., DAVIS R.J., DE BERNARDIS P., DE ROSA A., DE ZOTTI G., DELABROUILLE J., DICKINSON C., DIEGO J.M., DOLE H., DONZELLI S., DORE O., DOUSPIS M., DUCOUT A., DUPAC X., EFSTATHIOU G., ELSNER F., ENSSLIN T.A., ERIKSEN H.K., FALCETA-GONCALVES D., FALGARONE E., FERRIERE K., FINELLI F., FORNI O., FRAILIS M., FRAISSE A.A., FRANCESCHI E., FREJSEL A., GALEOTTA S., GALLI S., GANGA K., GHOSH T., GIARD M., GJERLOW E., GONZALEZ-NUEVO J., GORSKI K.M., GREGORIO A., GRUPPUSO A., GUDMUNDSSON J.E., GUILLET V., HARRISON D.L., HELOU G., HENNEBELLE P., HENROT-VERSILLE S., HERNANDEZ-MONTEAGUDO C., HERRANZ D., HILDEBRANDT S.R., HIVON E., HOLMES W.A., HORNSTRUP A., HUFFENBERGER K.M., HURIER G., JAFFE A.H., JAFFE T.R., JONES W.C., JUVELA M., KEIHANEN E., KESKITALO R., KISNER T.S., KNOCHE J., KUNZ M., KURKI-SUONIO H., LAGACHE G., LAMARRE J.-M., LASENBY A., LATTANZI M., LAWRENCE C.R., LEONARDI R., LEVRIER F., LIGUORI M., LILJE P.B., LINDEN-VORNLE M., LOPEZ-CANIEGO M., LUBIN P.M., MACIAS-PEREZ J.F., MAINO D., MANDOLESI N., MANGILLI A., MARIS M., MARTIN P.G., MARTINEZ-GONZALEZ E., MASI S., MATARRESE S., MELCHIORRI A., MENDES L., MENNELLA A., MIGLIACCIO M., MIVILLE-DESCHENES M.-A., MONETI A., MONTIER L., MORGANTE G., MORTLOCK D., MUNSHI D., MURPHY J.A., NASELSKY P., NATI F., NETTERFIELD C.B., NOVIELLO F., NOVIKOV D., NOVIKOV I., OPPERMANN N., OXBORROW C.A., PAGANO L., PAJOT F., PALADINI R., PAOLETTI D., PASIAN F., PEROTTO L., PETTORINO V., PIACENTINI F., PIAT M., PIERPAOLI E., PIETROBON D., PLASZCZYNSKI S., POINTECOUTEAU E., POLENTA G., PONTHIEU N., PRATT G.W., PRUNET S., PUGET J.-L., RACHEN J.P., REINECKE M., REMAZEILLES M., RENAULT C., RENZI A., RISTORCELLI I., ROCHA G., ROSSETTI M., ROUDIER G., RUBINO-MARTIN J.A., RUSHOLME B., SANDRI M., SANTOS D., SAVELAINEN M., SAVINI G., SCOTT D., SOLER J.D., STOLYAROV V., SUDIWALA R., SUTTON D., SUUR-USKI A.-S., SYGNET J.-F., TAUBER J.A., TERENZI L., TOFFOLATTI L., TOMASI M., TRISTRAM M., TUCCI M., UMANA G., VALENZIANO L., VALIVIITA J., VAN TENT B., VIELVA P., VILLA F., WADE L.A., WANDELT B.D., WEHUS I.K., YSARD N., YVON D. and ZONCA A.

Abstract (from CDS):

Within ten nearby (d<450pc) Gould belt molecular clouds we evaluate statistically the relative orientation between the magnetic field projected on the plane of sky, inferred from the polarized thermal emission of Galactic dust observed by Planck at 353GHz, and the gas column density structures, quantified by the gradient of the column density, NH. The selected regions, covering several degrees in size, are analysed at an effective angular resolution of 10' FWHM, thus sampling physical scales from 0.4 to 40pc in the nearest cloud. The column densities in the selected regions range from NH≃1021 to 1023cm–2, and hence they correspond to the bulk of the molecular clouds. The relative orientation is evaluated pixel by pixel and analysed in bins of column density using the novel statistical tool called ``histogram of relative orientations''. Throughout this study, we assume that the polarized emission observed by Planck at 353GHz is representative of the projected morphology of the magnetic field in each region, i.e., we assume a constant dust grain alignment efficiency, independent of the local environment. Within most clouds we find that the relative orientation changes progressively with increasing NH, from mostly parallel or having no preferred orientation to mostly perpendicular. In simulations of magnetohydrodynamic turbulence in molecular clouds this trend in relative orientation is a signature of Alfvenic or sub-Alfvenic turbulence, implying that the magnetic field is significant for the gas dynamics at the scales probed by Planck. We compare the deduced magnetic field strength with estimates we obtain from other methods and discuss the implications of the Planck observations for the general picture of molecular cloud formation and evolution.

Abstract Copyright: ∼

Journal keyword(s): ISM: general - ISM: magnetic fields - ISM: clouds - dust, extinction - submillimeter: ISM - infrared: ISM

Simbad objects: 20

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Number of rows : 20
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1364 0
2 Barnard 211 DNe 04 17 35 +27 43.1           ~ 127 0
3 Barnard 218 DNe 04 28.1 +26 16           ~ 37 0
4 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4415 0
5 NAME Orion Molecular Cloud MoC 05 56 -01.8           ~ 1098 1
6 NAME Chamaeleon Region SFR 11 55 -78.0           ~ 806 0
7 NAME Musca Cld 12 23 -71.3           ~ 221 0
8 NAME Lupus Complex SFR 16 03 -38.1           ~ 720 0
9 NAME Upper Sco-Cen As* 16 15 -24.2           ~ 1330 1
10 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3629 1
11 M 13 GlC 16 41 41.634 +36 27 40.75     5.8     ~ 2191 0
12 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 1100 2
13 NAME Aql Region reg 18 31.1 -02 10           ~ 391 0
14 NAME Aql Rift DNe 18 32 -01.0           ~ 316 1
15 NAME Corona Australis Cloud MoC 19 01 51 -36 58.9           ~ 490 0
16 NAME Cepheus Region reg 21 20 00.0 +72 30 00           ~ 113 0
17 IC 5146 OpC 21 53 29.3 +47 14 46           ~ 466 2
18 NAME Cepheus Cloud SFR 22 00.0 +76 30           ~ 145 0
19 NAME Cepheus Flare MoC 23 34 +72.0           ~ 128 0
20 NAME Gould Belt PoG ~ ~           ~ 873 1

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